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Mass and Age of Red Giant Branch Stars Observed with LAMOST and Kepler MNRAS 475, 3633–3643 (2018) doi:10.1093/mnras/stx3296 Advance Access publication 2017 December 22 Mass and age of red giant branch stars observed with LAMOST and Kepler Yaqian Wu,1‹ Maosheng Xiang,2‹† Shaolan Bi,1‹ Xiaowei Liu,3 Jie Yu,4,5 Marc Hon,6 Sanjib Sharma,4 Tanda Li,4,5,2 Yang Huang,3† Kang Liu,1 Xianfei Zhang,1 Downloaded from https://academic.oup.com/mnras/article-abstract/475/3/3633/4772882 by Sydney College of Arts user on 17 February 2019 Yaguang Li,1 Zhishuai Ge,1 Zhijia Tian,3† Jinghua Zhang1 and Jianwei Zhang1 1Department of Astronomy, Beijing Normal University, Beijing 100875, P. R. China 2National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, P. R. China 3Department of Astronomy, Peking University, Beijing 100871, P. R. China 4School of Physics, University of Sydney, Sydney 2000, NSW, Australia 5Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark 6School of Physics, The University of New South Wales, Sydney 2052, NSW, Australia Accepted 2017 December 19. Received 2017 December 19; in original form 2017 September 25 ABSTRACT Obtaining accurate and precise masses and ages for large numbers of giant stars is of great importance for unraveling the assemblage history of the Galaxy. In this paper, we estimate masses and ages of 6940 red giant branch (RGB) stars with asteroseismic parameters deduced from Kepler photometry and stellar atmospheric parameters derived from LAMOST spectra. The typical uncertainties of mass is a few per cent, and that of age is ∼20 per cent. The sample stars reveal two separate sequences in the age–[α/Fe] relation – a high-α sequence with stars older than ∼8 Gyr and a low-α sequence composed of stars with ages ranging from younger than 1 Gyr to older than 11 Gyr. We further investigate the feasibility of deducing ages and masses directly from LAMOST spectra with a machine learning method based on kernel based principal component analysis, taking a sub-sample of these RGB stars as a training data set. We demonstrate that ages thus derived achieve an accuracy of ∼24 per cent. We also explored the feasibility of estimating ages and masses based on the spectroscopically measured carbon and nitrogen abundances. The results are quite satisfactory and significantly improved compared to the previous studies. Key words: asteroseismology – stars: evolution – stars: fundamental parameters. (HRD) with the theoretical stellar isochrones, utilizing stellar at- 1 INTRODUCTION mospheric parameters yielded by spectroscopy and/or photometry. Accurate age estimates for large numbers of stars are important for a The method has been successfully applied to obtain reasonable age full understanding of the stellar populations and the assemblage his- estimates for a few thousand F/G type stars with high-resolution tory of the Galaxy. Age is one of the key parameters that determine spectroscopy (Edvardsson et al. 1993; Takeda 2007; Haywood et al. the evolutionary state of a star. However, unlike other parameters, 2013; Bergemann et al. 2014)orubvyβ photometry, compled with such as mass and chemical composition, direct age estimate for precise trigonometric parallax data (Nordstrom¨ et al. 2004). Re- a star from observation or fundamental physical law is extremely cently, Wu et al. (2017) used this method to obtain accurate ages for difficult if not impossible (e.g. Soderblom 2010). Often, one has about 200 main-sequence turn-off stars and used the results to check to rely on stellar evolutionary models for stellar age estimation – the accuracy of age estimation for tens of thousand main-sequence usually achieved by comparing the stellar parameters deduced from turn-off and subgiant stars targeted by the LAMOST spectroscopic the observation with the model predictions. surveys (Xiang et al. 2015a, 2017b). However, the method is diffi- A practical way of age estimation for individual field stars is cult to apply to giant stars, as isochrones of giants of different ages to compare their position on the Hertzsprung–Russell diagram are severely crowded together on the HRD, particularly in temper- ature. On the other hand, giant stars are advantaged probes of the Galactic structure as they can be detected to large distances given E-mail: [email protected] (YW); [email protected] (MX); their high luminosities. Modern large-scale surveys, such as the [email protected] (SB) LAMOST Galactic spectroscopic surveys (Deng et al. 2012;Zhao † LAMOST Fellow. et al. 2012) and the Apache Point Observatory Galactic Evolution C 2017 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society 3634 Y. Wu et al. Experiment (APOGEE; Majewski et al. 2010), have collected high- accurate parameters, stellar masses can be inferred to a precision of quality spectra that yield robust stellar atmospheric parameters and ∼7 per cent. About 14 000 stars spectra in the sample of Yu et al. chemical abundances for millions of giant stars. It has become an were targeted by LAMOST by 2016 June. Precise stellar parame- emergent task to develop an effective way that delivers robust age ters and elemental abundances, (e.g. [α/Fe], [C/H], and [N/H]), of estimates for large numbers of giant stars detected by the existing those stars were derived from the LAMOST spectra with the LSP3 and upcoming large spectroscopic surveys. (Xiang et al. 2015b, 2017a). Meanwhile, systematic errors of the Asteroseismologic studies have demonstrated that solar-like os- standard scaling relation were better assessed (White et al. 2011; cillations excited by convective turbulence in the stellar envelope Guggenberger et al. 2016;Sharmaetal.2016; Viani et al. 2017). Downloaded from https://academic.oup.com/mnras/article-abstract/475/3/3633/4772882 by Sydney College of Arts user on 17 February 2019 are always solar-like stars of 0.8–3.0 M (Aerts, Christensen- With these advantages, it seems that the time is ripe for better mass Dalsgaard & Kurtz 2010; Soderblom 2010; Chaplin & Miglio 2013). and age estimates for the large number of giants available from Both the grid modelling that fits the individual observed frequencies LAMOST surveys. (e.g. Chaplin et al. 2014) and a scaling relation based on global as- In this work, we determine masses and ages for the above teroseismic parameters, ν, the frequency separation of two modes LAMOST–Kepler common red giant branch (RGB) stars. The re- of the same spherical degree and consecutive radial order, and νmax, sults are shown to have a median error of 7 per cent in mass and frequency with the maximal oscillation power (Kjeldsen & Bedding 25 per cent in age estimates. With this LAMOST–Kepler sample, we 1995), have been used to infer mass and radius from the oscillation investigated possible correlations between stellar age and chemical data. Once the precise mass of a giant star has been determined, composition. We further selected a sub-sample of stars with smaller robust age, to an accuracy of about 20–30 per cent (e.g. Soderblom uncertainties in mass and age estimates as a training set to estimate 2010; Gai et al. 2011; Chaplin et al. 2014), then can be estimated by masses and ages directly from the LAMOST spectra with a ma- comparing the inferred mass with the theoretical stellar isochrones chine learning method based on kernel-based principal component of given metallicity, since the main-sequence lifetime of a star is analysis (KPCA). Feasibility of the method is discussed, and the tightly correlated with its mass (e.g. Martig et al. 2016; Ness et al. resultant age and mass estimates are compared with those inferred 2016). Precise photometry from the CoRoT (Baglin 2006), Kepler from an empirical relation based on the C and N abundances. We (Borucki et al. 2010), and K2 (Howell et al. 2014) space missions found that with the current approach, one can derive stellar ages has allowed determinations of seismic parameters for thousands of from the LAMOST spectra with a high precision of 23 per cent. red giant stars (e.g. De Ridder et al. 2009; Hekker et al. 2009, 2011; The paper is organized as follows. Section 2 introduces the Bedding et al. 2010;Mosseretal.2010; Stello et al. 2013, 2015, LAMOST–Kepler sample. Section 3 describes the mass and age es- 2017; Mathur et al. 2016;Yuetal.2016). Many of those stars have timation. Correlations between the age and elemental abundances also reliable atmospheric parameters yielded by spectroscopy, ei- are presented in Section 4. Section 5 presents ages and masses esti- ther from the literature (e.g. Huber et al. 2013; Chaplin et al. 2014; mated directly from the LAMOST spectra with the KPCA method. Pinsonneault et al. 2014), or targeted by the APOGEE (Majewski Section 6 discusses age and mass estimation based on the abundance et al. 2010)ortheLAMOST–Kepler surveys (De Cat et al. 2015), ratio [C/N], followed by conclusions is Section 7. so the ages of these stars can, in principle, be well-determined and adopted as benchmarks for age estimation for large numbers of 2 THE LAMOST–KEPLER SAMPLE giant stars detected in large-scale surveys. Martig et al. (2016) estimated mass and age for 1475 red giants 2.1 Atmospheric and asteroseismic parameters in the APOKASC sample that have atmospheric parameters and elemental abundances including [C/Fe] and [N/Fe] deduced from By 2016 June, the LAMOST–Kepler project (De Cat et al. 2015) APOGEE spectra, as well as seismic parameters derived from Ke- collected more than 180 000 low-resolution (R ∼ 1800) optical pler photometry (Pinsonneault et al. 2014). Based on the fact that spectra (λ 3800–9000 Å) in the Kepler field utilizing the LAMOST values of carbon and nitrogen abundance ratio [C/N] of red giant spectroscopic survey telescope (Cui et al.
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